Professori f m. f d. I. Sattorov ttymi qoshidagi al o‘qituvchisi L



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Tajriba guruhlari

Nazorat guruhlari

Bosqich

O’quvchilar

soni

Tajriba

guruhlarining

baholari

Sifat

tahlili

O’quvchilar

soni

Nazorat

guruhlari

baholari

Sifat

tahlili

Sifat

ko’rsatkichlari

farqi

5

4

3

2

5

4

3

2

1-

tajriva

31

12

12

7

-

77 %

29

4

11

14

-

52 %

26 %

2-

tajriba

27

9

13

5

-

81 %

30

6

8

16

-

47 %

34 %


Toshkent axborot texnologiyalari kasb-hunar kolleji



Tajriba guruhlari

Nazorat guruhlari

Bosqich

O’quvchilar

soni

Tajriba

guruhlarining

baholari

Sifat

tahlili

O’quvchilar

soni

g

Nazorat

uruhlari

aholari

Sifat

tahlili

Sifat

ko’rsatkichlari

farqi

5

4

3

2

5

4

3

2

1-

tajriva

32

7

15

10

-

69 %

32

4

9

16

3

41 %

28 %

2-

tajriba

30

8

17

5

-

83 %

30

5

7

14

4

37 %

46 %


Shunday q?ilib, tajriba guruhlaridagi o’quvchilarning bilim, amaliy ko’nikma darajalari nazorat guruhlaridagi o’quvchilarning bilim, amaliy ko’nikma darajalaridan katta ekanligi topildi.

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XULOSA

Ta’limda zamonaviy texnologiyalarni qo‘llash ta’lim sifatini oshirishda muhim o‘rin tutadi. Kadrlar tayyorlash milliy dasturini bajarilishi ta’lim sifatini oshirishni talab etadi. Shu munosabat bilan ta’limning turli yo‘nalishlariga zamonaviy texnologiyalar kirib kelmoqda.

Biz ushbu BMIda astronomiyada “Koinotning katta o‘lchamli tuzilishi” mavzusini kasb-hunar kollejlarida o‘qitish jarayoniga zamonaviy texnologiyalarni qo‘llash usullarni ko‘rsatib o‘tdik hamda mavzuga oid qator ilmiy adabiyotlarni tahlil qilib, o‘zlashtirdim.

Zamonaviy texnologiyalarni qo‘llash o‘quvchilarning faolligini oshiradi va shu orqali ularni chuqur bilim olishga undaydi. Shuningdek ularda olgan nazariy bilimlarni amalda qo‘llash ko‘nikmalarni shakllanishiga yordam beradi, ularda ijodiy qobiliyatlarini rivojlantiradi hamda mustaqil ishlash ko‘nikmasini shakllantiradi. Bular o‘z navbatida ularning kelgusida o‘z faoliyatlari davomida foydalanish imkoniyatini tug‘diradi.



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FOYDALANILGAN ADABIYOTLAR RO‘YXATI.



  1. Karimov.I.A. Barkamol avlod orzusi. Toshkent:Sharq 1998 -181. b.

  2. Karimov I. A. O‘zbekiston buyuk kelajak sari. Toshkent. O‘zbekiston, 1998. -691 b.

  3. Karimov I. A. Jamiyatimiz mafkurasi xalqni xalq, millatni millat qilishga xizmat etsin. //Tafakkur jurnali.- 1998.- №2. b. 24-26.

  4. «Kadrlar tayyorlashning milliy dasturi», Xalq ta’limi, 1998. №1, 5

  5. MapTbiHoB, В.Я., Курс oбщeй aстрoфизики, М., HayKa, 1986.

  6. Климишин И.А., Actpohomm ня^^^тих днeй, М., HayKa, 1980.

  7. Sattorov I., Yulduzlar nuri tilga kirganda, Toshkent, FAN, 1973.

  8. Sattorov I. Astrofizika, I qism, “IQTISOD-MOLIYA”, T., 2009

  9. Sattarova B. Koinotning uch o‘lchamli tuzilishi // Pedagogik ta’lim. - Toshkent, 2004. -№4. - B. 23-25.

  10. Sattarova B. Astronomiya kursida internet texnologiyaalari // Ta’limda ahborot kommunikatsiya texnologiyaalarini qo’llashning muammolari: Respublika ilmiy-amaliy konferentsiya materiallari. 23 may 2005. - Toshkent, 2005. - B. 53-,

  11. Sattarova B. Internet manbalaridan foydalanib astronomiyadan ma’ruza mash^ulotlariga tayyorlanish // Akademik litsey va kasb hunar kollejlarida fizika va matematika masalalarining dolzarb muammolari: Respublika ilmiy-amaliy konferentsiya materiallari. 27-28 oktyabr 2006. - Toshkent, 2006. - B. 187-190

  12. Sattarova B. Astronomik ta’limda ahborot texnologiyaalarini qo’llash zamon talabi // Fizika ta’limi taraqqiyoti va istiqbollari: Respublika ilmiy-amaliy konferentsiya materiallari. 23-24 may 2008. - Qarshi, 2008. - B. 82-83.

13.Sattarova B. Astronomiya. Kasb-hunar kollejlari o’qituvchilari uchun metodik qo’llanma. Toshkent. 2012.

14.Sattarov I. «Astrofizika» (2-qism, qo’llanma), Turon-Iqbol, T., 2007



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15.I.Sattorov, B.G‘.Qodirov, U.Sh.Begimqulov. «Astrofizikadan kompyutyerda laboratoriya ishlari». T.,Nizomiy nomidagi TDPU.,2002.

  1. Бакулин П.И.,Кононевич Э.В,Морзов В. И. « Курс общей астрономии». М., Наука, 1987.

  2. Климишин И. А. «Астрономия наших дней». М., Наука, 1990.

  3. http://festival.1 september.ru/arti cl es/s ubjects/3?page=3

  4. http: //www.astro galaxy.ru/296.html

  5. http://www.astro-web.ru/metod/media

  6. www.astronet.ru

  7. http: //en.wikipedia.org/wiki/College

  8. www.gettsburg.edu/CLEA , Internet sayti. 2003.

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1.

GALAKTIKA- GALAXY

A galaxy is a massive, gravitationally bound system that consists of stars and stellar remnants, an interstellar medium of gas dust, and an important but poorly understood component tentatively dubbed dark matter.The name is from the Greek word galaxias, literally meaning "milky", a reference to the Milky Way galaxy. Typical galaxies range from dwarfs with as few as ten million (107) stars, up to giants with a hundred trillion (1014) stars,[4] all orbiting the galaxy's center of mass. Galaxies may contain many star systems, star clusters, and various interstellar clouds. The Sun is one of the stars in the Milky Way galaxy; the Solar System includes the Earth and all the other objects that orbit the Sun.



2.

SPIRAL GALAKTIKA- SPIRAL GALAXY An example of a spiral galaxy, the Pinwheel Galaxy (also known as Messier 101 or NGC 5457)

A spiral galaxy is a certain kind of galaxy originally described by Edwin Hubble in his 1936 work The Realm of the Nebulae and, as such, forms part of the Hubble sequence. Spiral galaxies consist of a flat, rotating disk containing stars, gas and dust, and a central concentration of stars known as the bulge. These are surrounded by a much fainter halo of stars, many of which reside in globular clusters.

Spiral galaxies are named for the spiral structures that extend from the center into the disk. The spiral arms are sites of ongoing star formation and are brighter than the surrounding disk because of the young, hot OB stars that inhabit them.


3.

GALO- HALO

The galactic disk is surrounded by a spheroid halo of old stars and globular clusters, of which 90% lie within 100,000 light-years (30 kpc),[50] suggesting a stellar halo diameter of 200,000 light-years. However, a few globular clusters have been found farther, such as PAL 4 and AM1 at more than 200,000 light-years away from the galactic center. About 40% of these clusters are on retrograde orbits, which means they move in the opposite direction from the Milky Way rotation. The globular clusters can follow rosette orbits about the galaxy, in contrast to the elliptical orbit of a planet.

While the disk contains gas and dust which obscure the view in some wavelengths, the spheroid component does not. Active star formation takes place in the disk (especially in the spiral arms, which represent areas of high density), but not in the halo. Open clusters also occur primarily in the disk.

Discoveries in the early 21st century have added dimension to the knowledge of the Milky Way's structure. With the discovery that the disk of the Andromeda Galaxy (M31) extends much further than




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previously thought, the possibility of the disk of the Milky Way galaxy extending further is apparent, and this is supported by evidence from the discovery of the Outer Arm extension of the Cygnus Arm. With the discovery of the Sagittarius Dwarf Elliptical Galaxy came the discovery of a ribbon of galactic debris as the polar orbit of the dwarf and its interaction with the Milky Way tears it apart. Similarly, with the discovery of the Canis Major Dwarf Galaxy, it was found that a ring of galactic debris from its interaction with the Milky Way encircles the galactic disk.

4.

GALAKTIKA MARKAZI- GALACTIC CENTER

Main article: Galactic Center

Observed structure of the Milky Way's spiral arms. The Sun is in the Local Spur.

The galactic disc, which bulges outward at the galactic center, has a diameter of 70,000-100,000 light-years (20-30 kpc). The exact distance from the Sun to the galactic center is actively debated. The latest estimates from geometric-based methods and standard candles yield distances to the Galactic center of 7.6-8.7 kpc (25,000-28,000 ly). The fact that the estimates span over 1 kpc only underscores the true uncertainty associated with the distance to the Galactic center.

The galactic center harbors a compact object of very large mass as determined by the motion of material around the center. The intense radio source named Sagittarius A*, thought to mark the center of the Milky Way, is newly confirmed to be a supermassive black hole. Most galaxies are believed to have supermassive black holes at their centers.


5.

SPIRAL TARMOQLAR- SPIRAL ARMS Observed and extrapolated structure of the spiral arms.

Artist's conception of the spiral structure of the Milky Way with two major stellar arms and a bar.

Maps of the Milky Way's spiral structure are notoriously uncertain and exhibit striking differences. Some 150 years after Alexander (1852) first suggested that the Milky Way was a spiral, there is currently no consensus on the number or nature of the Galaxy's spiral arms. Perfect grand design logarithmic spiral patterns ineptly describe features near the Sun, namely since galaxies commonly exhibit arms that branch, merge, twist unexpectedly, and feature a degree of irregularity. The possible scenario of the Sun within a spur / Local arm emphasizes that point and indicates that such features are likely not unique, and exist elsewhere in the galaxy.


6.

GALAKTIKALARNI SINFLASHTIRISH- THE HUBBLE SEQUENCE IS A MORPHOLOGICAL CLASSIFICATION SCHEME FOR The Hubble sequence is a morphological classification scheme for galaxies invented by Edwin Hubble in 1926. It is often known colloquially as the Hubble tuning-fork diagram because of the shape in


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which it is traditionally represented.

Tuning-fork style diagram of the Hubble sequence Hubble’s scheme divides regular galaxies into 3 broad classes - ellipticals, lenticulars and spirals - based on their visual appearance (originally on photographic plates). A fourth class contains galaxies with an irregular appearance. To this day, the Hubble sequence is the most commonly used system for classifying galaxies, both in professional astronomical research and in amateur astronomy.



Edwin Hubble's Classification Scheme -


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